Birth of the Solar System

Lecture 42

Isotopic Anomalies in Meteorites

Isotopic variations, including those produced by extinct radionuclides, in meteorites tell us something about the

solar system’s prehistory

Neon Alphabet Soup• Neon isotopes could

originally be explained in terms of ‘solar’ (B), ‘planetary’ (A) and ‘spallogenic’ (S) components.

• New 22Ne-rich component, called Neon-E discovered in 1969 in step-heating.

• Found in 1988 to be contained in very fine SiC and graphite in Allende ground mass.o Ne-E(L), found in graphite, o Ne-E(H) in SiC. o The 20Ne/22Ne ratio of Ne-E(L) is less

than 0.01, while that of Ne-E(H) is less than 0.2.

Krypton & Xenon• Eventually, two

isotopically distinct components were identified: Xe-HL and the Xe-S component.o In what nucleosynthetic

environment are the heaviest and lightest isotopes on a element most likely to be synthesized?

• Supernova. • Carrier of Xe-HL

eventually identified as microdiamond (that of Xe-S as SiC). Xe-S and Ne-E derived from red giant.

Other anomalies• Once these interstellar grains were isolated, it

was possible to study their isotopic compositions in detail using ion microprobes.

• Once these interstellar grains were isolated, it was possible to study their isotopic compositions in detail using ion microprobes.

• Very large variations in the isotopic composition of carbon and nitrogen were found. The SiC grains do not form a single population, but represent a number of populations of grains, each produced in a different astronomical environment.

• Isotopic variations occur in a number of other elements, including Mg, Si, Ca, Ti, Sr, Zr, Mo, Ba, Nd, Sm, and Dy.

• The grains are clearly presolar - debris from red giants (which have very strong solar winds) and supernovae.

• First grains were ‘acid-resistant’ ones. Subsequently, presolar Si3N4, spinel, hibonite, a variety of metal carbides, TiO2, Fe-Ni metal and olivine were found.

• The extinct radionuclides indicate that some of this material had likely be synthesized shortly before the solar system formed.

Oxygen Isotope Anomalies

• O isotopes vary between all classes of meteorites - cannot be explained by mass dependent fractionation.o This is so systematic, O

isotopes can be used to classify meteorites.

• Earth & Moon share the same O isotopic composition as E-chondrites.

Oxygen Isotopes within Classes

• Variations within classes are mass dependent.

• Initially, nucleosynthetic cause was suspected.o Experimental demonstration of MIF variation

in ozone showed this need not be the case.

• Clayton (2002) suggested that the anomalies arose through radiation self-shielding in the solar nebula. o Ultraviolet radiation from the early protosun

dissociated carbon monoxide. Because C16O rather than C17O or C18O was the dominant oxygen-bearing species, this was quickly absorbed as it traveled outward from the Sun. At greater distance from the Sun only radiation of the frequency necessary to dissociate C17O and C18O would still be available. The O produced was then available to reaction with Si and other elements to form condensable solids.

o 16O-rich nature of the solar wind measured by Genesis spacecraft has now more or less verified this hypothesis.

Astronomical Constraints on Star

Formation

Star Birth• Star formation is more or less an everyday event

in the universe and we can watch it happening.• Stars form when fragments of large molecular

clouds collapse, as is occurring in the Great Nebula in Orion. Such clouds may have dimensions in excess of 106 AU and masses greater than 106 MO (solar masses).

• Gravity will tend to make such clouds collapse upon themselves, but is resisted by magnetic, rotational, and thermal forces.

• Collapse of a part of a nebula can occur through the removal of a supporting force, magnetic fields in particular, or by an increase in an external force, such as a passing shock wave, such as from a supernova or galactic arm.

• As the cloud collapses, it will warm adiabatically, resulting in thermal pressure that opposes collapse. Even small amounts of net angular momentum inherited from the larger nebula will cause the system to spin at an increasing rate as it contracts. For a cloud to collapse and create an isolated star, it must rid itself of over 99% of its angular momentum in the process of collapse. Otherwise the resulting centrifugal force will break up the star before it can form. Much of what occurs during early stellar evolution reflects the interplay between these factors.

Protostellar Evolution• Protostellar evolution of moderate-sized stars (i.e. stars similar

to the Sun) can be divided into 5 phases, based on the spectra of their electromagnetic emission & other observations.

• -I: initial collapse of a molecular cloud to form a nebular disk: no astronomical examples.o Once the cloud becomes optically dense the collapse slows. At this point, the protostellar

core has a radius of ~10 AU and a mass of ~1% of final mass. Further collapse brings the radius down to several times that of the eventual star in 106 to 107 years.

• 0: protostar deeply embedded in its cocoon of gas and dust and cannot be directly observed. At the beginning, the mass of the protostellar core is still very much smaller than that of the envelope of gas and dust. Angular momentum progressively flattens the envelope into a rotating disk. Material from the surrounding envelope continues to accrete to the disk, but mass is also transferred from the disk to the protostar.

Young Stars in Orion

Phase I• Phase I: L1551 IRS5 in Taurus a good

example. Two protostars about 45 AU apart with a combined mass of about 1 MO deeply embedded in circumstellar disks that have diameters of about 20 AU. However, surface temperatures of the disks range from 50 to 400 K at 1 AU. Models that reproduce these surface temperatures have disk interior temperatures that ranging 200 to 1500 K at 1 AU.

• The highest temperatures, which are enough to vaporize silicates, are likely short-lived and persist only for a period of perhaps 105 yr during which accretion rates are highest. More moderate temperatures, in the range of 200–700 K, could persist in the inner part of the disk for substantially longer than this.

• A very interesting feature of Class I objects is strong “bipolar flows” perpendicular to the disks that extend some 1000 AU. Within these jets, temperatures may locally reach 100,000 K. As the high velocity material in the jets collides with the interstellar medium it creates a shock wave that in turn generate X-rays.

X-Wind Model• In the X-wind model, the bipolar

outflows are the cores of a much broader outflow that emerges from the innermost part of the circumstellar disk as it interacts with the strong magnetic field of the central protostar. Shang et al. (2000):o “in the X-wind model, the combination of strong

magnetic fields and rapid rotation of the young star-disk system acts as an ‘eggbeater’ to whip out part of the material from the surrounding disk while allowing the rest to sink deeper in the bowl of the gravitational potential well”. The jets and associated X-wind remove both mass and angular momentum from the system.

• X-wind model provides a potential mechanism for cycling dust very close to the star where it might be almost completely evaporated, then blown back out into the nebula.

Phase II: T-Tauri Phase• Phase II is represented by so-called classical T-Tauri

stars, of which the star T-Tauri (now known to be a binary pair) is the type example. During this phase, a visible star begins to emerge from its cocoon of gas and dust, but it remains surrounded by its circumstellar disk.

• The luminosity is due entirely to continued accretion and gravitational collapse – fusion has not yet ignited in its interior. A T-Tauri star of one solar mass would have a diameter still several times that of the Sun.

• X-ray bursts from these stars suggest a more active surface than that of mature stars, likely driven by strong stellar magnetic fields and their interaction with the accretion disk.

• The surrounding disk is still warm enough to give off measurable IR radiation.

• Accretion to the star has dropped to rates of 10-6 to 10-8 MO per year. Bipolar outflows and associated X-wind continue. Typical mass loss rates from the flows and winds are 10-8 MO per year.

• Both Class I and II objects can go through occasional “FU Orionis outbursts” in which the disk outshines the central star by factors of 100–1000, and a powerful wind emerges, producing mass losses of 10-6 MO per year. These outbursts are thought to be the result of greatly enhanced mass accretion rates, perhaps as high as 10-4 MO per year.

Hubble Space Telescope views of the T-Tauri star DG Tau B. Left: Near Infrared Camera and Multi-Object Spectrometer, Right is taken with the Wide Field Planetary Camera. The accretion disk is a dark horizontal band in both images. Infrared interferometry indicates there is a gap of about 0.25 AU between the star and the inner edge of the disk, which extends out about 100 AU.

Phase III• Represented by weak-lined T-Tauri stars, so called because spectral

emission and absorption lines are much weaker and excess infrared emission is absent. The inference is that the disk has largely dissipated by this stage. Like classical T-Tauri stars, weak-lined T-Tauri stars are cooler yet more luminous than mature main sequence stars of similar mass, but they are closer to the main sequence on the Hertzsprung-Russell diagram than classical T-Tauris.

• Weak-lined T-Tauris are particularly luminous in the X-ray part of the spectrum. These X-rays are thought to be produced in hot plasma during magnetic reconnection events above the stellar surface. flares of weak-lined T-Tauris are 100–1000 times more powerful than solar flares produced in a similar way.

• Outflows and winds subside to those of typical main sequence stars as accretion ends and the star reaches its final mass. During the weak-lined T-Tauri phase, the star contracts to its final radius and density.

• At the end of this process, fusion ignites in the core and the luminosity and temperature of the star settles onto the main sequence. The entire process from Phase 0 through Phase III consumes perhaps 10 million years.

Beta-Pictoris

disk appears to be clearing from the inside out.